CN104977024A - Solar blind ultraviolet remote sensing camera absolute radiometric calibration coefficient in-orbit correction method - Google Patents

Abstract

The present invention relates to a solar blind ultraviolet camera absolute radiometric calibration equation coefficient in-orbit correction method, wherein a camera is subjected to laboratory absolute radiometric calibration to obtain the absolute radiometric calibration coefficient and the non-uniformity correction coefficient of the camera, the atmosphere background radiation value calculated based on the atmosphere radiation transmission model can be considered as the true background radiance when the camera in-orbit operating meets a certain constraint of the imaging mode, the location and the illumination condition, the background radiance is inverted according to the laboratory absolute radiometric calibration coefficient and the image local gray mean, and a linear regression method is used to analyze the inverted radiance value and the true radiance value so as to achieve the in-orbit correction of the calibration equation coefficient. According to the present invention, according to the solar blind ultraviolet spectrum atmosphere background radiation characteristic, the high-frequency and operational in-orbit absolute radiometric calibration of the solar blind ultraviolet spectrum remote sensor can be supported, and the blank of the in-orbit absolute radiometric calibration method of the domestic camera at the spectrum is filled.

Description

On-orbit correction method for absolute radiometric calibration coefficient of solar blind ultraviolet remote sensing camera

Technical Field

The invention relates to an on-orbit correction method for an absolute radiometric calibration coefficient of a solar blind ultraviolet remote sensing camera, and belongs to the technical field of aerospace optical remote sensing.

Background

From the 20 th century, the United states reflected OGO-4(1976), S3-4(1978), DE-1(1981), VIKING (1986), Polar BEAR (1986), and AURA (2004) for remote sensing of atmospheric gases in the Ultraviolet spectrum, most of which used on-orbit absolute radiometric Calibration Using UV Stars, such as the single-point absolute radiometric Calibration mentioned in Calibration of the Viking atomic Imager Using ultra Star, Satellite Observations with the VUI Instrument, et al, which had two problems: firstly, determining a proportionality coefficient between camera response and star radiant flux density by imaging a star point target, and using the method for radiometric calibration to assume that a camera response characteristic curve meets a proportionality relationship y which is k.x, namely, considering that the offset of an absolute radiometric calibration equation of the camera is 0, and if the offset is not established, a large radiometric calibration error can be brought; secondly, because ultraviolet star radiation scaling belongs to point scaling, and because of the influence of a point spread function PSF of a camera system, a point target is imaged on an image surface to form a diffuse spot, the size of the diffuse spot is related to the flare angle of the target to the system and the PSF, and errors are inevitably introduced in the statistics of the total radiance of the diffuse spot.

Disclosure of Invention

The technical problem solved by the invention is as follows: the method is characterized in that linear regression analysis is carried out on entrance pupil radiance inverted according to a laboratory absolute radiometric calibration equation and background radiance calculated according to a camera imaging mode and a radiation transmission theoretical model, and correction of the ground radiometric calibration equation coefficient is achieved.

The technical scheme of the invention is as follows: an on-orbit correction method for absolute radiation calibration coefficients of solar blind ultraviolet cameras comprises the following steps:

(1) carrying out radiometric calibration in a laboratory to obtain an absolute radiometric calibration equation and a non-uniform correction coefficient;

11) camera absolute radiometric calibration

Adjusting the radiance of the camera light source from small to large to L in turn₁,L₂……L_N(L₁<L₂<……<L_N) Corresponding to an average response of the camera output of, in turnObtaining a group of laboratory calibration point sequences by adopting least square normal linear fitting:

<math> <mrow> <mi>L</mi> <mo>=</mo> <mi>KV</mi> <mo>+</mo> <mi>C</mi> <mrow> <mo>(</mo> <mover> <msub> <mi>V</mi> <mn>1</mn> </msub> <mo>&OverBar;</mo> </mover> <mo>&le;</mo> <mi>V</mi> <mo>&le;</mo> <mover> <msub> <mi>V</mi> <mi>N</mi> </msub> <mo>&OverBar;</mo> </mover> <mo>)</mo> </mrow> <mo>;</mo> </mrow> </math>

where K and C are fitting coefficients, the average response of the camera outputAnd substituting the equation in sequence to calculate the radiance L value, and calculating the camera average response lower calibration residual:

<math> <mrow> <msub> <mi>&epsiv;</mi> <mi>i</mi> </msub> <mo>=</mo> <mfrac> <mrow> <mi>L</mi> <mo>-</mo> <msub> <mi>L</mi> <mi>i</mi> </msub> </mrow> <msub> <mi>L</mi> <mi>i</mi> </msub> </mfrac> <mo>=</mo> <mfrac> <mrow> <mi>k</mi> <mover> <msub> <mi>V</mi> <mi>i</mi> </msub> <mo>&OverBar;</mo> </mover> <mo>+</mo> <mi>c</mi> <mo>-</mo> <msub> <mi>L</mi> <mi>i</mi> </msub> </mrow> <msub> <mi>L</mi> <mi>i</mi> </msub> </mfrac> <mo>;</mo> </mrow> </math>

checking in turn whether each point calibration residual satisfies-_i|<If the number of the calibration points is not 5%, the calibration points are removed from the calibration points, otherwise, the calibration points are reserved, the reserved calibration points form a new calibration point sequence, if the removal of the calibration points occurs in the inspection, least square linear fitting and inspection calibration residual errors are repeated on the new calibration point sequence until the removal of the calibration points does not occur in the inspectionPoint, the equation obtained by the least square normal fitting at this time is a camera absolute radiometric calibration equation:

<math> <mrow> <mi>L</mi> <mo>=</mo> <mi>KV</mi> <mo>+</mo> <mi>C</mi> <mrow> <mo>(</mo> <msub> <mover> <mi>V</mi> <mo>&OverBar;</mo> </mover> <mi>min</mi> </msub> <mo>&le;</mo> <mi>V</mi> <mo>&le;</mo> <msub> <mover> <mi>V</mi> <mo>&OverBar;</mo> </mover> <mi>max</mi> </msub> <mo>)</mo> </mrow> <mo>;</mo> </mrow> </math>

the fitting coefficients K and C are camera absolute radiometric calibration coefficients, representing gain and bias respectively,to scale the minimum average response of the point sequence,to scale the maximum average response of the point sequence,is the camera linear response range;

12) pixel absolute radiometric calibration

According to the camera absolute radiometric calibration method, pixel-by-pixel absolute radiometric calibration is carried out on the camera, and the obtained camera pixel absolute radiometric calibration equation is as follows:

L＝k_i,jv_i,j+c_i,j；

wherein v is_i,jRepresenting the response, k, of the picture element (i, j)_i,jAnd c_i,jRepresents the gain and bias of the picture element (i, j);

13) non-uniformity correction

The calculation formula of the non-uniformity correction coefficient is as follows:

$G_{i,j}=\frac{k_{i,j}}{K}$

<math> <mrow> <msub> <mi>Q</mi> <mrow> <mi>i</mi> <mo>,</mo> <mi>j</mi> </mrow> </msub> <mo>=</mo> <mo>-</mo> <mfrac> <mi>C</mi> <mi>K</mi> </mfrac> <mo>+</mo> <msub> <mi>G</mi> <mrow> <mi>i</mi> <mo>,</mo> <mi>j</mi> </mrow> </msub> <mo>&CenterDot;</mo> <mfrac> <msub> <mi>c</mi> <mrow> <mi>i</mi> <mo>,</mo> <mi>j</mi> </mrow> </msub> <msub> <mi>k</mi> <mrow> <mi>i</mi> <mo>,</mo> <mi>j</mi> </mrow> </msub> </mfrac> <mo>;</mo> </mrow> </math>

wherein G is_i,jAnd Q_i,jNon-uniformity correction coefficients, i.e., non-uniformity correction gain and non-uniformity correction offset;

(2) acquiring the on-orbit imaging parameters of the camera, including imaging mode and imaging time T₁The number of satellite orbits (a, e, i, omega, M)₀) And an in-orbit image;

(3) judging whether the on-orbit imaging mode of the camera is the off-satellite point imaging, if so, entering the step (4), otherwise, jumping back to the step (2) to obtain new on-orbit imaging parameters of the camera again;

(4) according to the imaging time T₁And satelliteThe number of orbits (a, e, i, omega, M)₀) Calculating to obtain the geographical latitude of the satellite lower point

(5) Judgment of T₁Whether the time satellite is located in a middle latitude area or not is judged according to the following criteria:

if the criterion condition is met, entering the step (6), otherwise, jumping back to the step (2) to obtain new camera in-orbit imaging parameters again;

(6) calculating to obtain T₁Solar altitude h of satellite subsatellite point at moment_s

Wherein,₀indicating declination of the sun, phi is the latitude of the point under the star,is the solar hour angle;

(7) judgment of T₁Whether the satellite meets the illumination condition at the moment is judged as follows:

h_s>20°；

if the criterion condition is met, entering the step (8), otherwise, jumping back to the step (2) to obtain new camera in-orbit imaging parameters again;

(8) according to T₁Time satellite intersatellite point latitudeSun altitude h of the points below the star_sCalculating to obtain the entrance pupil radiance of the camera

(9) And relatively non-uniformly correcting the on-orbit image by the following correction formula:

V_i,j＝G_i,j×v_i,j+Q_i,j；

v_i,jas a response value before the rail image correction, V_i,jThe corrected response value of the on-track image is obtained;

(10) according to the ground resolution a multiplied by b of the camera, calculating and obtaining the maximum scaling area line number N for the background radiance inversion_aAnd number of columns N_b：

$N_a=\left[\frac{50}{a}\right]$

$N_b=\left[\frac{50}{b}\right];$

Wherein [. ]]Representing rounding; taking the central pixel of the on-orbit image after non-uniform correction as the center, and intercepting the image with the size of N_row×N_colRectangular region of (2), N_row、N_colAre positive integers with value ranges of N_row≤N_aAnd N_col≤N_bCalculating to obtain the average gray value of the image in the intercepted calibration area

(11) Judging the average gray value of the imageWhether the response is in the linear range or not is judged by the following criteria:

<math> <mrow> <msub> <mover> <mi>V</mi> <mo>&OverBar;</mo> </mover> <mi>min</mi> </msub> <mo>&lt;</mo> <msubsup> <mi>V</mi> <mi>orbit</mi> <mi>T</mi> </msubsup> <mo>&lt;</mo> <msub> <mover> <mi>V</mi> <mo>&OverBar;</mo> </mover> <mi>max</mi> </msub> <mo>;</mo> </mrow> </math>

if the criterion condition is met, inverting the entrance pupil radiance according to the camera absolute radiance scaling coefficients K and C

$L_{\mathrm{calibration}}^T=(V_{\mathrm{orbit}}^T-C)/K;$

Otherwise, jumping back to the step (2) to obtain new camera on-orbit imaging parameters again;

(12) change observation time to T in sequence₁,T₂,…T_mM is a positive integer larger than 2, and the entrance pupil radiance sequence of the camera is calculated according to the steps (3) to (8)According to the corresponding absolute radiometric calibration coefficient and image average response of the cameraInverting the entrance pupil according to the steps (9) to (11)Radiance sequenceObtaining a coefficient K of a unary linear regression equation by least square normal fitting_orbitAnd C_orbit：

L_orbit＝K_orbitL_calibration+C_orbit；

(13) And (3) correcting the camera absolute radiometric calibration equation obtained in the step (1) by using the unitary linear regression equation coefficient obtained in the step (12), and obtaining a corrected absolute radiometric calibration equation:

L＝K_orbitKV+K_orbitC+C_orbit；

wherein K_orbitK is the gain, K_orbitC+C_orbitIs an offset.

Compared with the prior art, the invention has the advantages that:

(1) the existing foreign solar blind ultraviolet remote sensing camera single-point on-orbit absolute radiation calibration method based on the ultraviolet fixed star has the following defects:

a) the single-point method can only determine a gain value, and if the offset exists in the response of the machine in the whole dynamic range, the radiation calibration precision of the single-point method cannot be ensured;

b) the ultraviolet fixed star is a point target, the point target is imaged as a diffuse spot on an image surface due to the influence of a point spread function PSF of a camera system, the size of the diffuse spot is related to the field angle of the target to the system and the PSF, the total radiance of the diffuse spot can represent the ultraviolet radiation characteristic of the fixed star, and errors are inevitably introduced by the statistics of the total radiance;

the invention overcomes the defects of the existing on-orbit absolute radiation calibration of the solar blind ultraviolet remote sensing camera, and provides a correction method of the on-orbit absolute radiation calibration equation coefficient of the general solar blind ultraviolet spectral band camera based on atmospheric background observation under the constraint condition for the first time;

(2) based on the atmospheric background radiation characteristic of the solar blind ultraviolet spectrum, the calculation result of the atmospheric radiation transmission model can be used as the real background radiance under the observation constraint conditions of an imaging mode, an imaging area and a lighting condition by adopting the idea of cross radiometric calibration, and the coefficient correction of the on-orbit absolute radiometric calibration equation only depends on the laboratory absolute radiometric calibration result and the on-orbit atmospheric background image of the camera, so that the method is easy to implement and popularize in the engineering, and the high-frequency on-orbit calibration requirement of the remote sensing camera can be met;

(3) the achievement of the invention can provide technical reference for the on-orbit absolute radiation calibration of the domestic solar blind spectral band remote sensor.

Drawings

Fig. 1 is a comparison graph of calculation of a LOWTRAN 7 model and on-orbit actual measurement of solar blind ultraviolet background radiance of an S3-4 satellite ultraviolet camera at a solar altitude of 24 degrees, wherein an abscissa represents wavelength, an ordinate represents spectral radiance, a solid line in the graph is the spectral radiance calculated by the model, and a dotted line is the on-orbit actual measurement spectral radiance;

FIG. 2 is a flow chart of the method of the present invention.

Detailed Description

The characteristics of solar blind ultraviolet atmosphere background radiation are analyzed as follows:

1) the on-orbit actual measurement result of the American CIPS solar blind ultraviolet imaging detector shows that: the atmospheric background solar blind ultraviolet radiation has the characteristic of uniform spatial distribution, and the brightness change of the atmospheric background radiation within the range of 50km multiplied by 50km of the point under the satellite is less than 5 per thousand;

2) the comparison result of the theoretical calculation model of atmospheric background radiance in the solar blind ultraviolet spectrum and the measurement of a space-based ultraviolet camera shows that: the in-orbit atmospheric background radiation measurement result of the solar blind ultraviolet band is highly consistent with an atmospheric radiation transmission model LOWTRAN theoretical calculation model, fig. 1 shows a comparison graph of LOWTRAN 7 model calculation and in-orbit actual measurement solar blind ultraviolet background radiance of an S3-4 satellite ultraviolet camera at a solar altitude angle of 24 degrees, the abscissa represents wavelength, the ordinate represents spectral radiance, wherein the solid line is a model calculation value, and the dotted line is an in-orbit actual measurement value. The consistency requires that the ultraviolet camera on-track measurement meets the following three observation conditions:

i. the observation mode of the detector is imaging of a point under the satellite;

a solar elevation angle of the sub-satellite point is greater than 20 degrees;

the geographical latitude of the sub-satellite region is the mid-latitude region;

3) the result of calculating the atmospheric background radiance of the solar blind ultraviolet spectrum by using LOWTRAN simulation shows that: the radiance of the atmospheric background at the satellite points is only related to the zenith angle of the sun, the seasons and the geographical positions of the satellite points, and is not related to other atmospheric conditions such as the reflectivity of ground objects, visibility, cloud and rain conditions and the like.

Based on the analysis result, an on-orbit correction method for the absolute radiometric calibration coefficient of the solar blind ultraviolet remote sensing camera is provided: under the constraint of certain camera observation conditions, calculating atmospheric background radiation by radiation transmission software to serve as an on-orbit real measurement value, performing linear regression analysis on the atmospheric background radiation and a radiance value inverted according to a laboratory calibration equation, and correcting the coefficients of the laboratory absolute radiation calibration equation, as shown in fig. 1:

(1) carrying out radiometric calibration in a laboratory to obtain an absolute radiometric calibration equation and a non-uniform correction coefficient;

11) absolute radiometric calibration

Setting working parameters of a camera, and adjusting the radiance of a light source of the camera from small to large to L in sequence₁,L₂……L_N(L₁<L₂<……<L_N) Corresponding to an average response of the camera output of, in turnObtaining a group of laboratory calibration point sequences by adopting least square normal linear fitting:

<math> <mrow> <mi>L</mi> <mo>=</mo> <mi>KV</mi> <mo>+</mo> <mi>C</mi> <mrow> <mo>(</mo> <mover> <msub> <mi>V</mi> <mn>1</mn> </msub> <mo>&OverBar;</mo> </mover> <mo>&le;</mo> <mi>V</mi> <mo>&le;</mo> <mover> <msub> <mi>V</mi> <mi>N</mi> </msub> <mo>&OverBar;</mo> </mover> <mo>)</mo> </mrow> <mo>;</mo> </mrow> </math>

where K and C are fitting coefficients, the average response of the camera outputAnd substituting the equations in sequence to calculate the radiance L value, and calculating the camera average response lower calibration residual:

<math> <mrow> <msub> <mi>&epsiv;</mi> <mi>i</mi> </msub> <mo>=</mo> <mfrac> <mrow> <mi>L</mi> <mo>-</mo> <msub> <mi>L</mi> <mi>i</mi> </msub> </mrow> <msub> <mi>L</mi> <mi>i</mi> </msub> </mfrac> <mo>=</mo> <mfrac> <mrow> <mi>k</mi> <mover> <msub> <mi>V</mi> <mi>i</mi> </msub> <mo>&OverBar;</mo> </mover> <mo>+</mo> <mi>c</mi> <mo>-</mo> <msub> <mi>L</mi> <mi>i</mi> </msub> </mrow> <msub> <mi>L</mi> <mi>i</mi> </msub> </mfrac> <mo>;</mo> </mrow> </math>

the nonlinear response characteristics of the low end and the high end of the camera are considered, in order to ensure the radiometric calibration precision of a laboratory, the following method is adopted to remove nonlinear calibration points, and the radiance corresponding to the removed calibration points can be subjected to radiometric calibration processing under other camera working parameters.

Checking in turn whether each point calibration residual satisfies-_i|<And 5%, if the absolute radiation calibration equation does not meet the standard, eliminating the calibration point from the calibration point, otherwise, reserving the calibration point, forming a new calibration point sequence by the reserved calibration points, if the calibration point is eliminated in the current inspection, repeating least square linear fitting and inspection calibration residual error on the new calibration point sequence, and otherwise, obtaining the equation by the least square normal linear fitting:

<math> <mrow> <mi>L</mi> <mo>=</mo> <mi>KV</mi> <mo>+</mo> <mi>C</mi> <mrow> <mo>(</mo> <msub> <mover> <mi>V</mi> <mo>&OverBar;</mo> </mover> <mi>min</mi> </msub> <mo>&le;</mo> <mi>V</mi> <mo>&le;</mo> <msub> <mover> <mi>V</mi> <mo>&OverBar;</mo> </mover> <mi>max</mi> </msub> <mo>)</mo> </mrow> <mo>;</mo> </mrow> </math>

the fitting coefficients K and C are camera absolute radiometric calibration coefficients, representing gain and bias respectively,to scale the minimum average response of the point sequence,to scale the maximum average response of the point sequence,is the camera linear response range;

12) pixel absolute radiometric calibration

According to the camera absolute radiometric calibration method, pixel-by-pixel absolute radiometric calibration is carried out on the camera, and the obtained camera pixel absolute radiometric calibration equation is as follows:

L＝k_i,jv_i,j+c_i,j；

wherein v is_i,jRepresenting the response, k, of the picture element (i, j)_i,jAnd c_i,jRepresents the gain and bias of the picture element (i, j);

13) non-uniformity correction

The calculation formula of the non-uniformity correction coefficient is as follows:

$G_{i,j}=\frac{k_{i,j}}{K}$

<math> <mrow> <msub> <mi>Q</mi> <mrow> <mi>i</mi> <mo>,</mo> <mi>j</mi> </mrow> </msub> <mo>=</mo> <mo>-</mo> <mfrac> <mi>C</mi> <mi>K</mi> </mfrac> <mo>+</mo> <msub> <mi>G</mi> <mrow> <mi>i</mi> <mo>,</mo> <mi>j</mi> </mrow> </msub> <mo>&CenterDot;</mo> <mfrac> <msub> <mi>c</mi> <mrow> <mi>i</mi> <mo>,</mo> <mi>j</mi> </mrow> </msub> <msub> <mi>k</mi> <mrow> <mi>i</mi> <mo>,</mo> <mi>j</mi> </mrow> </msub> </mfrac> <mo>;</mo> </mrow> </math>

wherein G is_i,jAnd Q_i,jNon-uniformity correction coefficients, i.e., non-uniformity correction gain and non-uniformity correction offset;

(2) acquiring the on-orbit imaging parameters of the camera, including imaging mode and imaging time T₁The number of satellite orbits (a, e, i, omega, M)₀) And an in-orbit image;

(3) judging whether the on-orbit imaging mode of the camera is the off-satellite point imaging, if so, entering the step (4), otherwise, jumping back to the step (2) to obtain new on-orbit imaging parameters of the camera again;

(4) according to the imaging time T and the number of satellite orbits (a, e, i, omega, M)₀) Calculating satellite subsatellite point geographic latitude

41) Calculating a deviation angle E of the T moment

Iterative solution of Kepler's equation

E_i+1＝M+e sin E_i；

Wherein e is eccentricity and M is a mean-near point angle; when | E_i+1-E_i|<Taking E as E_i+1(ii) a For a given precision, the initial value of the iteration takes E₁＝M；

42) Calculating the true approach point angle f at the moment T

$\tan \frac{f}{2}=\sqrt{\frac{1+e}{1-e}}\tan \frac{E}{2};$

WhereinAndin the same quadrant;

43) calculating the center-to-earth distance r at the moment T

$r=\frac{a(1-e^2)}{1+e\cos f};$

Wherein a is a semi-major axis;

44) computing latitude argument u at T moment

u＝ω+f；

Wherein omega is the argument of the perigee;

45) calculating the position x, y, z of the satellite at the T moment in the celestial coordinate system

x＝r(cosΩcos u-sinΩsin u cos i)

y＝r(sinΩcos u+cosΩsin u cos i)

z＝r sin u sin i；

Wherein omega is the right ascension of the ascending crossing point;

46) calculating the longitude and latitude alpha and phi of the satellite subsatellite point at the T moment

<math> <mrow> <mi>sin</mi> <mi>&phi;</mi> <mo>=</mo> <mfrac> <mi>Z</mi> <mi>r</mi> </mfrac> </mrow> </math>

47) Calculating satellite subsatellite point geographic latitude at T moment

(5) Judgment of T₁Whether the time satellite is located in a middle latitude area or not is judged according to the following criteria:

if the criterion condition is met, entering the step (6), otherwise, jumping back to the step (2) to obtain new camera in-orbit imaging parameters again;

(6) calculating T₁Solar altitude h of satellite subsatellite point at moment_s

Wherein,₀indicating declination of the sun, phi is the latitude of the point under the star,is the solar hour angle;

(7) judgment of T₁Whether the satellite meets the illumination condition at the moment is judged as follows:

h_s>20°；

if the criterion condition is met, entering the step (8), otherwise, jumping back to the step (2) to obtain new camera in-orbit imaging parameters again;

(8) according to T₁Time satellite intersatellite point latitudeSun altitude h of the points below the star_sCalculating the entrance pupil radiance of the camera

(9) And relatively non-uniformly correcting the on-orbit image by the following correction formula:

V_i,j＝G_i,j×v_i,j+Q_i,j；

v_i,jas a response value before the rail image correction, V_i,jThe corrected response value of the on-track image is obtained;

(10) calculating the number of scaling area lines N which can be used for the inversion of the background radiance at most according to the ground resolution a x b of the camera and the unit of the ground resolution km_aAnd number of columns N_b：

$N_a=\left[\frac{50}{a}\right]$

$N_b=\left[\frac{50}{b}\right];$

Wherein [. ]]Representing rounding; intercepting the image with the size of N by taking the central pixel of the on-orbit image after non-uniform correction as the center_row×N_colRectangular region of (2), N_row、N_colAre positive integers with value ranges of N_row≤N_aAnd N_col≤N_bCalculating the average gray value of the image in the intercepted calibration area

(11) Judging the average gray value of the imageWhether the response is in the linear range or not is judged by the following criteria:

<math> <mrow> <msub> <mover> <mi>V</mi> <mo>&OverBar;</mo> </mover> <mi>min</mi> </msub> <mo>&lt;</mo> <msubsup> <mi>V</mi> <mi>orbit</mi> <mi>T</mi> </msubsup> <mo>&lt;</mo> <msub> <mover> <mi>V</mi> <mo>&OverBar;</mo> </mover> <mi>max</mi> </msub> <mo>;</mo> </mrow> </math>

if the criterion condition is met, inverting the entrance pupil radiance according to the camera absolute radiance scaling coefficients K and C

$V_{\mathrm{calibration}}^T=(V_{\mathrm{orbit}}^T-C)/K;$

Otherwise, jumping back to the step (2) to obtain new camera on-orbit imaging parameters again;

(12) change observation time to T in sequence₁,T₂,…T_mM is a positive integer larger than 2, and the entrance pupil radiance sequence of the camera is calculated according to the steps (3) to (8)According to the corresponding absolute radiometric calibration coefficient and image average response of the cameraAnd (4) inversely calculating a camera entrance pupil radiance sequence according to the steps (9) to (11)Obtaining a coefficient K of a unary linear regression equation by least square normal fitting_orbitAnd C_orbit：

L_orbit＝K_orbitL_calibration+C_orbit；

(13) And (3) correcting the camera absolute radiometric calibration equation obtained in the step (1) by using the unitary linear regression equation coefficient obtained in the step (12), and obtaining a corrected absolute radiometric calibration equation:

L＝K_orbitKV+K_orbitC+C_orbit；

wherein K_orbitK is the gain, K_orbitC+C_orbitIs an offset.

Those skilled in the art will appreciate that the details of the present invention not described in detail herein are well within the skill of those in the art.

Claims (1)

1. An on-orbit correction method for absolute radiation calibration coefficients of solar blind ultraviolet cameras is characterized by comprising the following steps:

(1) carrying out radiometric calibration in a laboratory to obtain an absolute radiometric calibration equation and a non-uniform correction coefficient;

11) camera absolute radiometric calibration

Adjusting the radiance of the camera light source from small to large to L in turn₁,L₂……L_N(L₁<L₂<……<L_N) Corresponding to an average response of the camera output of, in turnObtaining a group of laboratory calibration point sequences by adopting least square normal linear fitting:

<math> <mrow> <mi>L</mi> <mo>=</mo> <mi>KV</mi> <mo>+</mo> <mi>C</mi> <mrow> <mo>(</mo> <msub> <mover> <mi>V</mi> <mo>&OverBar;</mo> </mover> <mn>1</mn> </msub> <mo>&le;</mo> <mi>V</mi> <mo>&le;</mo> <msub> <mover> <mi>V</mi> <mo>&OverBar;</mo> </mover> <mi>N</mi> </msub> <mo>)</mo> </mrow> <mo>;</mo> </mrow> </math>

where K and C are fitting coefficients, the average response of the camera outputAnd substituting the equation in sequence to calculate the radiance L value, and calculating the camera average response lower calibration residual:

<math> <mrow> <msub> <mi>&epsiv;</mi> <mi>i</mi> </msub> <mo>=</mo> <mfrac> <mrow> <mi>L</mi> <mo>-</mo> <msub> <mi>L</mi> <mi>i</mi> </msub> </mrow> <msub> <mi>L</mi> <mi>i</mi> </msub> </mfrac> <mo>=</mo> <mfrac> <mrow> <mi>k</mi> <msub> <mover> <mi>V</mi> <mo>&OverBar;</mo> </mover> <mi>i</mi> </msub> <mo>+</mo> <mi>c</mi> <mo>-</mo> <msub> <mi>L</mi> <mi>i</mi> </msub> </mrow> <msub> <mi>L</mi> <mi>i</mi> </msub> </mfrac> <mo>;</mo> </mrow> </math>

checking each point in turn the scaled residual isWhether satisfy-_i|<And 5%, if the absolute radiation calibration equation does not meet the requirement, eliminating the calibration point from the calibration point, otherwise, reserving the calibration point, forming a new calibration point sequence by the reserved calibration points, if the elimination of the calibration point occurs in the inspection, repeating least square linear fitting and inspection calibration residual error on the new calibration point sequence until the elimination of the calibration point does not occur in the inspection, and obtaining the equation by the least square normal fitting at the time as the camera absolute radiation calibration equation:

<math> <mrow> <mi>L</mi> <mo>=</mo> <mi>KV</mi> <mo>+</mo> <mi>C</mi> <mrow> <mo>(</mo> <msub> <mover> <mi>V</mi> <mo>&OverBar;</mo> </mover> <mi>min</mi> </msub> <mo>&le;</mo> <mi>V</mi> <mo>&le;</mo> <msub> <mover> <mi>V</mi> <mo>&OverBar;</mo> </mover> <mi>max</mi> </msub> <mo>)</mo> </mrow> <mo>;</mo> </mrow> </math>

the fitting coefficients K and C are camera absolute radiometric calibration coefficients, representing gain and bias respectively,to scale the minimum average response of the point sequence,to scale the maximum average response of the point sequence,is the camera linear response range;

12) pixel absolute radiometric calibration

According to the camera absolute radiometric calibration method, pixel-by-pixel absolute radiometric calibration is carried out on the camera, and the obtained camera pixel absolute radiometric calibration equation is as follows:

L＝k_i,jv_i,j+c_i,j；

wherein v is_i,jRepresentation imageResponse of element (i, j), k_i,jAnd c_i,jRepresents the gain and bias of the picture element (i, j);

13) non-uniformity correction

The calculation formula of the non-uniformity correction coefficient is as follows:

$G_{i,j}=\frac{k_{i,j}}{K}$

<math> <mrow> <msub> <mi>Q</mi> <mrow> <mi>i</mi> <mo>,</mo> <mi>j</mi> </mrow> </msub> <mo>=</mo> <mo>-</mo> <mfrac> <mi>C</mi> <mi>K</mi> </mfrac> <mo>+</mo> <msub> <mi>G</mi> <mrow> <mi>i</mi> <mo>,</mo> <mi>j</mi> </mrow> </msub> <mo>&CenterDot;</mo> <mfrac> <msub> <mi>c</mi> <mrow> <mi>i</mi> <mo>,</mo> <mi>j</mi> </mrow> </msub> <msub> <mi>k</mi> <mrow> <mi>i</mi> <mo>,</mo> <mi>j</mi> </mrow> </msub> </mfrac> <mo>;</mo> </mrow> </math>

wherein G is_i,jAnd Q_i,jNon-uniformity correction coefficients, i.e., non-uniformity correction gain and non-uniformity correction offset;

(2) acquiring the on-orbit imaging parameters of the camera, including imaging mode and imaging time T₁The number of satellite orbits (a, e, i, omega, M)₀) And an in-orbit image;

(3) judging whether the on-orbit imaging mode of the camera is the off-satellite point imaging, if so, entering the step (4), otherwise, jumping back to the step (2) to obtain new on-orbit imaging parameters of the camera again;

(4) according to the imaging time T₁And the number of satellite orbits (a, e, i, omega, M)₀) Calculating to obtain the geographical latitude of the satellite lower point

(5) Judgment of T₁Whether the time satellite is located in a middle latitude area or not is judged according to the following criteria:

if the criterion condition is met, entering the step (6), otherwise, jumping back to the step (2) to obtain new camera in-orbit imaging parameters again;

(6) calculating to obtain T₁Solar altitude h of satellite subsatellite point at moment_s

Wherein,₀indicating declination of the sun, phi is the latitude of the point under the star,is the solar hour angle;

(7) judgment of T₁Whether the satellite meets the illumination condition at the moment is judged as follows:

h_s>20°；

if the criterion condition is met, entering the step (8), otherwise, jumping back to the step (2) to obtain new camera in-orbit imaging parameters again;

(8) according to T₁Time satellite intersatellite point latitudeSun altitude h of the points below the star_sCalculating to obtain the entrance pupil radiance of the camera

(9) And relatively non-uniformly correcting the on-orbit image by the following correction formula:

V_i,j＝G_i,j×v_i,j+Q_i,j；

v_i,jas a response value before the rail image correction, V_i,jThe corrected response value of the on-track image is obtained;

(10) according to the ground resolution a multiplied by b of the camera, calculating and obtaining the maximum scaling area line number N for the background radiance inversion_aAnd number of columns N_b：

$\begin{array}{c}{N}_a=\left[\frac{50}{a}\right]\\ N_b=\left[\frac{50}{b}\right]\end{array};$

Wherein [. ]]Representing rounding; taking the central pixel of the on-orbit image after non-uniform correction as the center, and intercepting the image with the size of N_row×N_colRectangular region of (2), N_row、N_colAre positive integers with value ranges of N_row≤N_aAnd N_col≤N_bCalculating to obtain the average gray value of the image in the intercepted calibration area

(11) Judging the average gray value of the imageWhether the response is in the linear range or not is judged by the following criteria:

<math> <mrow> <msub> <mover> <mi>V</mi> <mo>&OverBar;</mo> </mover> <mi>min</mi> </msub> <mo>&lt;</mo> <msubsup> <mi>V</mi> <mi>orbit</mi> <mi>T</mi> </msubsup> <mo>&lt;</mo> <msub> <mover> <mi>V</mi> <mo>&OverBar;</mo> </mover> <mi>max</mi> </msub> <mo>;</mo> </mrow> </math>

if the criterion condition is met, inverting the entrance pupil radiance according to the camera absolute radiance scaling coefficients K and C $L_{\mathrm{calibration}}^T:$

$L_{\mathrm{calibration}}^T=(V_{\mathrm{orbit}}^T-C)/K;$

Otherwise, jumping back to the step (2) to obtain new camera on-orbit imaging parameters again;

(12) change observation time to T in sequence₁,T₂,…T_mM is a positive integer larger than 2, and the entrance pupil radiance sequence of the camera is calculated according to the steps (3) to (8)According to the corresponding absolute radiometric calibration coefficient and image average response of the cameraInverting the entrance pupil radiance sequence according to the steps (9) to (11)Obtaining a coefficient K of a unary linear regression equation by least square normal fitting_orbitAnd C_orbit：

L_orbit＝K_orbitL_calibration+C_orbit；

(13) And (3) correcting the camera absolute radiometric calibration equation obtained in the step (1) by using the unitary linear regression equation coefficient obtained in the step (12), and obtaining a corrected absolute radiometric calibration equation:

L＝K_orbitKV+K_orbitC+C_orbit；

wherein K_orbitK is the gain, K_orbitC+C_orbitIs an offset.